Planets before 1995…

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You are here!

Planets before 1995…

small rocky planets close to the Sun

gas-giant planets more distant from the star

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IRIS / Voyager R = 4.3 cm-1 Voyager /UVS

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• Solving mass continuity equation

– –

– Kzz = K0n^-,   0.5

• Temperature profile from thermochemical calculation

• Chemical reactions from, for example, Yung and DeMore (1999)

i i zz i

i i

atm zz i

i i zz i

i

i nw

T K D z

n T H

K H

n D K

z D

n + + +

¶ - ¶ +

-

¶ + -¶

= (1 ) ]

[ )

( )

( a

j

i i i

i P L

z t

n = -

¶ + ¶

¶

¶ j

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Solar system:

small rocky planets close to the Sun gas-giant planets more distant from the star  

Sun

51 Pegas: a gas-giant very close to its parent star (hot- Jupiter)

() M. Mayor & D. Queloz, 1995, Nature 378 p. 355

51 Peg

51 Peg b

Mercury Venus Earth

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Radial velocity + Transit Surveys Radial velocity + Transit Surveys

(Corot, Kepler, ground) (Corot, Kepler, ground)

Microlensing, direct detec.

GAIA -> 10

GAIA -> 10⁴⁴ new planets! new planets!

~700 Exoplanets!

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12

More than 1200 planetary candidates discovered by

Kepler!

Exoplanets are common…

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Mayor & Queloz, 1995

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Deming et al., 2005 Charbonneau et al.,

2005

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Microlensing

Beaulieu et al., 2005

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Direct detection Direct detection

10⁹ photons in the visible

10⁶ photons in the infrared

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Where are those planets?

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The lightest

1.9 Earth masses (Gliese581d) The heaviest

+5000 Earth masses (HD 202206 b) The shortest year

1 day + 5 hours (OGLE-TR-56 b) The longest year

100 years (PSR B1620-26 b) The closest to the Earth 10 light years (Epsilon Eridani)

The farest to the Earth

22000 light years (OGLE-390 b)

1 light-year = 10 000 billion km

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Equal opportunity for Super- Equal opportunity for Super-

Earths

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Sertorio & Tinetti, 2002 Williams et al., 2002

Duffy, Tinetti, Liang, in prep

Combining eccentricity and tilt

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Transit lightcurve

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Transit of the planet with the longest year:

from ULO

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Transit hunters Transit hunters

Earth-size planet transiting Sun-type star ~ 0.01 %

COROT (CNES/ESA) launch Dec. 2006

Corot 7b, First transiting super Earth Kepler (NASA)

launch 2009

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Taken from Bill Borucki’ s 25 presentation

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Taken from Bill Borucki’ s presentation

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Taken from Bill Borucki’ s 27 presentation

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Radial velocity & Occultation

Period = 3.524738 days Period = 3.524738 days

Mass = 0.69 ±0.05 M

Mass = 0.69 ±0.05 M_Jupiter_Jupiter

Radius = 1.35 ±0.04 Radius = 1.35 ±0.04 RR_Jupiter_Jupiter

Density = 0.35 ±0.05 Density = 0.35 ±0.05 g/cmg/cm³³

HD 209458b

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Sotin, Grasset & Mocquet;

Kuchner & Seager;

Ice

Silicate Carbon

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Galileo « Sidereus Nuncius » 1610 Galileo (the mission), 1989

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Kipping, 2008, 2009, 2010, 2011;

Kipping et al., 2009;

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Charbonneau et al.,

2009; Winn et al., 2011

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There is more to mass and radius…

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41

Neptune/GJ436

Kepler 10b

CoRoT-7b

GJ1214

Earth

A new class of planets with masses between the Earth mass and the 10 Earth masses

–“ Super-Earths” – seem to be quite common but absent from our Solar System

55 Cnc e

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artist’s impressions!

Are they Habitable?

Mayor et al., 2009;

Wordsworth et al, 2011

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GJ 581d (model)

Wordsworth et al. (2011)

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Hanel et al. (1970)

The acquisition of

spectroscopic data of the Earth from artificial

satellites has changed the old question of whether

the phenomenon of

terrestrial life is unique or not…

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IRIS / Voyager R = 4.3 cm-1

Samuelson et al. (1983)

Titan

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Planet with no atmosphere

= _

R _p = R

(47)

= _

R _p = R

Planet with no

atmosphere

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= _

R _p = R

Planet with no

atmosphere

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R _p = R

R _p = R’ R _p = R’’

=

_

=

_

=

_

(50)

Spectral signature of a Spectral signature of a

transiting planet transiting planet

R

_p²

/R

_s²



Molecule a Molecule b Planetary limb~0.01-0.1%

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Secondary transit – emission spectroscopy

Time

Flux

~ F_p/F_s(R_p²/R_s²)

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Flux

Wavelength

Individual lightcurves

Different transit depths

Spectral signature of an exoplanet

Time

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Borucki et al., 2009 Knutson et al., 2007 HD189733b

Spitzer

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Combined light star-

planet

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Harrington et al., Science, 2006

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Hubble-STIS

589. nm Wavelength (nm)

0.0232±0.0057

%

0.0131±0.0038

%

Na in the atmosphere of Hot- Jupiters

Charbonneau et al., 2002

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STIS: Ly

STIS: Lyaa HD 209458b HD 209458b

~9% absorption in the Ly

~9% absorption in the Lyaa line, line,

No red/blue shiftNo red/blue shift

Ben-Jaffel, ApJL, 2008

15% absorption in the Lya line

Vidal-Madjar et al., Nature, 2003 Ballester, Sing, Herbert, Nature,

2007

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CII Transit Measurements

(Linsky et al. 2010)

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SiIII Transit Measurements

(Linsky et al. 2010)

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STIS: Ly

STIS: Lyaa HD 209458b HD 209458b

Planetary properties of the upper Planetary properties of the upper

atmosphere

atmosphere Stellar wind

Koskinen et al., 2010; Yelle, 2003;

Lecavelier et al., 2003; Lammer..2004, Tian et al. 2005,

Koskinen et al., Nature, 2008 Holmstrom et al., Nature, 2008

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UV Science case

•Atoms and Ions.

Such observations may thus provide the best constraints on elemental abundance ratios (e.g., O/H, C/H, N/H) of these atmospheres.

•Mass Loss

The mass loss rates is determined by chemistry and dynamics in the upper

atmosphere that is driven by the UV flux of the host star. UV transit observations can be used to constrain the velocity profile of the escaping gas and thus mass loss rates.

•Star UV fluxes

The UV flux is the driver of photochemistry in the stratosphere/mesosphere region.

Most current models of photochemistry and dynamics in the upper atmosphere use unreliable scaling laws to simulate the fluxes of stars

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O₃

200 250 300

Tropopause Stratopause

Water Vapor

Ozone Absorption

Absorption 0

10 20 30 40 50 60

Net

Emission

Multiple scattering of reflected photons:

Rayleigh

scattering/clouds/surface types. Molecules with

electronic transitions

Photons emitted by the planet,

Molecules (roto- vibrational modes), thermal structure, clouds

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Water in HD 209458b

Barman, 2007; Knutson et al., 2007 Barman, 2007; Knutson et al., 2007

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Tinetti et al., Nature, 2007;

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Tinetti et al., Nature, 2007;

Beaulieu et al., 2009

Terminator of

HD189733b & HD209458b

Burrows et al., 2010

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Grillmair et al., Nature, 2008

HD189733b, day-side

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Swain, Vasisht, Tinetti, Nature, 2008

HD189733b, terminator

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Hubble + Spitzer legacy

HD189733b, terminator

Tinetti and Griffith, 2010

NICMOS,

Swain et al., 2008

Beaulieu et al., 2008 Desert et al., 2009

Agol et al., 2008

Knutson et al., 2008

H₂O, CH₄, CO₂ /CO?

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Methane-rich atmosphere?

Hubble, Spitzer, ground…

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Methane-rich atmosphere?

No evidence of CO/CO₂

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Degeneracy of solutions

Stevenson et al., Nature, 2010

Methane-rich atmosphere or methane poor?

Spectroscopy needed!

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HD189733b, day-side

Swain et al, 2009

CO₂

CH₄ H₂O

CH₄

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Transit spectroscopy, Hubble

Tinetti, et al., 2010

XO-1b

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Tinetti, et al., 2010

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A non-parametric machine learning algorithm

Waldmann, ApJ, 2011

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Waldmann, ApJ, 2011

A non-parametric machine learning algorithm

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87

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Na-K in the atmosphere of Hot-

JupitersGround-based observations

Redfield et al., 2007; Snellen et al., 2008; Sing et al., 2010

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Carbon Monoxide?

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CO detection with VLT-Crires CO detection with VLT-Crires

Snellen et al., Nature, 2010

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91

Super-Earth: GJ 1214b

~6 Earth masses, 450K

Bean et al., Nature, 2010

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Non –LTE emission at 3.25 microns in HD 189733b

IRTF K-band IRTF L-

band Spitzer/IRA

C

Swain et al. Nature, 2010

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Non –LTE methane emission at 3.25 microns

Drossart et al. 1999

Swain et al. 2010

HD 189733b

Cassini fly-by

Titan Jupiter

Saturn

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Ground based facilities we use

IRTF, Hawaii, 3.0 meters TNG, La Palma, 3.58 metersMMT, Arizona, 4.8 meters

WHT, La Palma, 4.2 meters VLT, Chile, 8.2 meters LBT, Arizona, 8.4 meters

HD189733b GJ1214b / WASP 12b GJ1214b

GJ1214b HD198733b/HD209458b

WASP18b / GJ1214b

WASP 33b

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NASA Infrared Telescope Facility (IRTF)

• 3.0 m primary mirror

• Mauna Kea

• optimized for NIR

SpeX instrument:

• Cross dispersion grism

• 1.9 – 4.2 microns

• Medium resolution R ~ 2000

K-band L-band

What we do from the ground:

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96

Step1: Removing the telescope systematics

Before cleaningAfter cleaning

TIME

WAVELENGTH Waldmann et al in prep.

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Swain et al. Nature 2010

HD 189733b – L band ground based spectroscopy

12^th August 2007 Swain et al. Nature 2010

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Swain et al. Nature 2010, Waldmann et al. 2011 12^th August 2007 12^th August 2007

Swain et al. Nature 2010 Waldmann et al. in prep.

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12^th August 2007 12^th August 2007 22^nd June 2009

Swain et al. Nature 2010, Waldmann et al. 2011

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12^th August 2007 12^th August 2007 22^nd June 2009 12^th July 2009

Swain et al. Nature 2010, Waldmann et al 2011.

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HD189733b, transmission spectroscopy

Waldmann et al., ApJ, 2011

Ground-base spectroscopic observations

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Methane fluorescence scheme

Non-LTE model by Drossart

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Danielski et al., in prep.

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Models & Degeneracy of solutions

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Inverse models

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(AIRS data)

Mid-lat

Polar Desert

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Swain, et al., 2009; Griffith and Tinetti, 2010

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HD209458b, day-side

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Madhu & Seager, 2009;

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Automatic spectral retrieval

Lee, Fletcher, Irwin, 2011;

Line et al., 2011

From NEMESIS retrieval code

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EChO

Exoplanet Characterisation Observatory

ESA M3 mission candidate – assessment phase

ESA Science Team

G. Tinetti

P. Drossart

O. Krause

C. Lovis

G. Micela

M. Ollivier

I. Ribas

I. Snellen

B. Swinyard

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 EChO selected as ESA-M3, Feb.

2011

 ESA internal study finished (thumbs up, technically)

 Payload consortium proposal submitted:

UK, France, Italy, Spain, Denmark, Germany, Un. Liege, US

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Planets studied by EChO

Temperature

Radius

‘ Hot’

(850-1500K)

‘ Warm’

(500-800K)

‘ Habitable Zone’

(250-350K)

Jupiter Neptun e

Super Earth

(119)

Temperature

Radius

‘ Hot’

(850-1500K)

‘ Warm’

(500-800K)

(250-350K)

Jupiter Neptun e

Super Earth

Tessenyi et al., ApJ, in press

(120)

Temperature

Radius

‘ Hot’

(850-1500K)

‘ Warm’

(500-800K)

(250-350K)

Jupiter Neptun e

Super Earth

Easy Easy OK

Easy/? Easy OK

Low

Resolution Low

Resolution Low Resolution / bright late stars

Tessenyi et al., ApJ, in press

(121)

EChO proposal, 2010

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EChO proposal, 2010

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EChO proposal, 2010

(124)

Habitable-zone for different stars

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Tessenyi et al, ApJ, in press

(126)

Tessenyi et al, ApJ, in press

(127)

Molecules observed by EChO

EChO proposal, 2010

(128)

Venus phases, Galileo

(129)

EChO performances

(130)

Planets observed by EChO today & in 2020

EChO proposal, 2010; Tinetti et al., 2011

(131)

Repetita Iuvant: atmospheric dynamics

Cho et al, 2006

(132)

Atmospheric chemistry

Moses et al, 2010

(133)

We find water vapour, methane, CO, COWe find water vapour, methane, CO, CO₂₂ present in the Hot-Jupiters analysed

present in the Hot-Jupiters analysed

There is a degeneracy of interpretation There is a degeneracy of interpretation mixing ratios/thermal profiles.

mixing ratios/thermal profiles.

More data at higher resolution are More data at higher resolution are desirable to break the degeneracy desirable to break the degeneracy

 and also better line lists for methane, and also better line lists for methane, hydrocarbons, H

hydrocarbons, H₂₂S, etc. @ 1000-2000KS, etc. @ 1000-2000K

Favorable Neptunes and Super-Earths can Favorable Neptunes and Super-Earths can already been studied with transit technique already been studied with transit technique

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Join the EChO team!

Help us designing the best possible mission

Planets before 1995…

Planets before 1995…

~700 Exoplanets!

More than 1200 planetary candidates discovered by

Kepler!

Exoplanets are common…

Microlensing

Direct detection Direct detection

Where are those planets?

Where are those planets?

Equal opportunity for Super- Equal opportunity for Super-

Earths

Earths

Combining eccentricity and tilt

Transit lightcurve

Transit of the planet with the longest year:

from ULO

Transit hunters Transit hunters

Radial velocity & Occultation

HD 209458b

HD 209458b

There is more to mass and radius…

Are they Habitable?

Are they Habitable?

GJ 581d (model)

Titan

Planet with no atmosphere

= 

R p = R

= 

R p = R

Planet with no

atmosphere

= 

R p = R

Planet with no

atmosphere

R p = R

R p = R’ R p = R’’

=

=

=

Spectral signature of a Spectral signature of a

transiting planet transiting planet

R

/R



Combined light star-

planet

Hubble-STIS

Na in the atmosphere of Hot- Jupiters

CII Transit Measurements

(Linsky et al. 2010)

SiIII Transit Measurements

(Linsky et al. 2010)

UV Science case

Water in HD 209458b

HD189733b, day-side

HD189733b, terminator

HD189733b, terminator

Methane-rich atmosphere?

Hubble, Spitzer, ground…

Degeneracy of solutions

HD189733b, day-side

XO-1b

Carbon Monoxide?

Carbon Monoxide?

CO detection with VLT-Crires CO detection with VLT-Crires

Super-Earth: GJ 1214b

~6 Earth masses, 450K

Ground based facilities we use

Inverse models

HD209458b, day-side

Automatic spectral retrieval

EChO

Habitable-zone for different stars

Venus phases, Galileo

Join the EChO team!

= _

R _p = R

= _

R _p = R

= _

R _p = R

R _p = R

R _p = R’ R _p = R’’